Astronomy and Astrophysics – Astrophysics – Galaxy Astrophysics
Scientific paper
2011-03-31
Astronomy and Astrophysics
Astrophysics
Galaxy Astrophysics
11 pages, 11 figures, accepted for publication in MNRAS. For high-resolution figures ask the authors
Scientific paper
We analyse for the first time the radial abundance gradients of the disc stars of a disc galaxy simulated with our three dimensional, fully cosmological chemodynamical galaxy evolution code GCD+. We study how [Fe/H], [N/O], [O/Fe], [Mg/Fe] and [Si/Fe] vary with galactocentric radius. For the young stars of the disc, we found a negative slope for [Fe/H] and [N/O] but a positive [O/Fe], [Mg/Fe] and [Si/Fe] slope with radius. By analysing the star formation rate (SFR) at different radii, we found that the simulated disc contains a greater fraction of young stars in the outer regions, while the old stars tend to be concentrated in the inner parts of the disc. This can explain the positive [alpha/Fe] gradient as well as the negative [N/O] gradient with radius. This radial trend is a natural outcome of an inside-out formation of the disc, regardless of its size and can thus explain the recently observed positive [alpha/Fe] gradients in the Milky Way disc open clusters.
Allende Prieto Carlos
Brook Chris B.
Gibson Brad K.
Kawata Daisuke
Kiessling Alina
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